What is EDGE?

EDGE is a project to numerically simulate the very smallest galaxies in the Universe. It is an international collaboration spearheaded by the University of Surrey (PI Prof. Justin Read), Durham University and the University of Lund. The simulations are set up using the new GenetIC initial conditions generator and run using the RAMSES code. Analysis of simulation outputs is performed using the AHF halo finder in addition to both PyNbody and Tangoes analysis tools. The EDGE simulations are run on the DiRAC High Performance Computing Facility which is hosted across the UK and has been awarded more than 175 Mcpu hours.

While EDGE is an international effort, we would not be here without the hard work of all who put in their time to work on these simulations. For a full list of amazing people apart of EDGE please see the Collaborators page.

Features of EDGE

While EDGE possesses two suites with differing physics packages, there are many core aspects of the EDGE prescription that have remained the same between them. Some of which are detailed here, if you would like a full description of the physics included in either EDGE suite then see the physics description page.

Dark Matter Resolution

Dark matter particles within 5 virial radii of a target halo are targeted to be 118 M, and 944 M within hires and fiducial level simulations respectively.

Galaxy Mass Range

Isolated dwarf galaxies are selected to possess a halo mass within the range of 108-10 M hosting stellar masses 105-7 M.

Star Particle Resolution

Star particles form self consistently from dense cold gas (300mp/cc,<100k) and are single stellar populations (SSPs) representative of a group of stars formed from a single star formation event. Particles Sample a Kroupa IMF with a mass of 300 M.

Stellar Feedback

Stellar winds and supernovae are both modelled within the simulations. MORE DETAILS

Grid Resolution

Increasing densities cause the grid to undergo refinement in regions of interest. We target a max level of refinement of 3pc within both hires and fiducial level simulations.

Complete Merger Histories

Both suites possess large box sizes (50 Mpc3 for EDGE1 suite, and 100 Mpc3 for EDGE2) resulting in a full cosmological merger history of target systems.

The Science

Aliquam diam consequat

Eget mattis at, laoreet vel amet sed velit aliquam diam ante, dolor aliquet sit amet vulputate mattis amet laoreet lorem.

EDGE: A New Model for Nuclear Star Cluster Formation in Dwarf Galaxies

In this paper, we investigate the formation of simulated dwarf galaxies that play host Nulear Star Clsters, additionally we study their observational properties, and compare them to observed Globular Clusters such as Omega-Centuri.

Mattis tempus lorem

Eget mattis at, laoreet vel amet sed velit aliquam diam ante, dolor aliquet sit amet vulputate mattis amet laoreet lorem.